Neutron Cooper pairs [1]}, which comprise a major component of the
nuclear matter in a pulsar, form a superfluid. Therefore,
Refs. [2]}, [3]} have proposed simply to model
this superfluid by using the two-dimensional (2D) Gross-Pitaevskii equation
(GPE); in addition, they have included an externally imposed potential or
container and a pinning potential for the crust.
However, pulsars are three dimensional (3D); and gravitational effects are
important on stellar scales. It is important, therefore, to account for these
crucial features in a model for pulsars and the glitches they exhibit. In this
Letter, we construct a natural, minimal model for pulsar glitches by
(a) accounting for gravitational effects via the Gross-Pitaevskii-Poisson equation
(GPPE) for a self-gravitating superfluid (see, e.g.,
Refs. [4]}, [5]}, [6]} for a non-rotating bosonic star)
and (b) including rotation and an interacting solid crust.
